Computer Science – Numerical Analysis
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.253..193p&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 253, Nov. 15, 1991, p. 193-197.
Computer Science
Numerical Analysis
46
Photosphere, Stellar Atmospheres, Stellar Luminosity, Stellar Spectra, X Ray Spectra, X Ray Stars, Analytic Functions, Electron Energy, Numerical Analysis, Stellar Models
Scientific paper
Numerical and analytical models of photospheres of X-ray bursts have been developed for the case when the burster luminosity is very close to the Eddington limit, l = L/L(Ed) = 0.9-0.999. It is shown that the burst spectrum at observable energies can be described by a diluted Wien spectrum with the spectral temperature T coinciding with the electron temperature in an isothermal outer layer formed by Compton heating in the neutron star photosphere. The dilution factor is proportional to (Teff/T) exp 4, where Teff is the effective temperature. Simple expressions are obtained for T/Teff, and for the dilution factor, which are determined by the parameter (1 - l)/(3 + 5X), where X is the hydrogen abundance. Fitting spectra observed around peaks of strong bursts may put additional constraints on masses and radii of neutron stars, and give new information on chemical composition of their photospheres and on distances to the bursters.
Pavlov George G.
Shibanov Iu. A.
Zavlin Vyacheslav E.
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